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REVIEW 4 major objections 5 minor 1 cited by

Two Dynamical Scenarios for Binned Master Sample Interpretation

T0 review · 4 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read An interacting dark energy model, with a mildly phantom equation of state, best reproduces the decreasing effective Hubble constant seen in the binned Master supernova sample.

desk verdict A tunable parameter fixed to match the target makes the DE-DM 'preference' circular, but the clean setup and the DE negative result justify a referee shot. read the letter →

arxiv 2507.14048 v2 pith:P3YSLBYQ submitted 2025-07-18 astro-ph.CO gr-qc

Giovanni Montani , Elisa Fazzari , Nakia Carlevaro , Maria Giovanna Dainotti This is my paper
classification astro-ph.COgr-qc PACS 98.80.-k
keywords HubbletensiondarkenergyinteractingTypeIasupernovaerunningconstantbinnedMastersamplepower-lawMCMC
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

The paper pits two late-universe models against the binned 'Master' sample of Type Ia supernovae: a pure evolutionary dark energy model, in which dark energy is created by the expanding universe's gravitational field, and a model in which that created dark energy also interacts with matter. Using the effective running Hubble constant $H_0(z)$ as diagnostic, an MCMC analysis finds the data overwhelmingly prefer the interacting model; the non-interacting model is strongly disfavored relative to a power-law reference ($\Delta\mathrm{BIC}=6.6$). Fixing the interacting model's flat dark energy parameter to $-1.0073$ makes it reproduce the decreasing power-law $H_0(z)$ with residuals below $0.15\%$. The paper's case is that dark energy–matter interaction is a viable dynamical explanation for the redshift-dependent Hubble constant behind the tension.

What carries the argument

The diagnostic that carries the comparison is the effective running Hubble constant $H_0(z) \equiv H(z)/\sqrt{\Omega_{m0}(1+z)^3 + 1 - \Omega_{m0}}$, which maps each model's expansion history onto the same observable plotted against binned SNe Ia redshifts. The physical mechanism is gravitational particle creation: a rate $\Gamma = \Gamma_* H \rho_{\mathrm{de}}^{-\alpha}$ (set to $\alpha=1$) lets the expanding universe's gravitational field create dark energy, with creation suppressed as $\rho_{\mathrm{de}}$ grows. In the interacting version, the sum of matter and dark energy energy-momentum tensors is conserved, coupling the two densities and letting matter drain away faster than in $\Lambda$CDM, which produces the declining $H_0(z)$. The statistical machinery is a standard MCMC sampling over uniform priors followed by BIC comparison against the power-law reference.

What would settle it

Re-derive $H_0(z)$ from the Master sample using an unbinned likelihood or a binning scheme that explicitly corrects for selection biases; if the decreasing power-law trend disappears or changes materially, the DE-DM model's match to that trend would be a fit to a statistical artifact, and the central claim would collapse.

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Extended reading notes

Core claim

On its own terms, the paper establishes that a model with dark energy creation by the gravitational field plus a dark energy–matter interaction, described by joint conservation of the two energy-momentum tensors, yields an effective running Hubble constant that matches the decreasing power-law trend previously fitted to the 20-bin Master sample ($H_0(z)=H_0(1+z)^a$ with $a=0.010$, $H_0=69.869\,\mathrm{km\,s^{-1}\,Mpc^{-1}}$). The match is achieved by setting $w_{\mathrm{de}}=-1.0073$, a mildly phantom equation of state, and the residuals between the model curve and the power-law reference are less than $0.15\%$. In contrast, the pure evolutionary dark energy model without interaction is strongly disfavored ($\Delta\mathrm{BIC}=6.6$). The paper concludes that dark energy interacting with matter, like $f(R)$ gravity, can reproduce a monotonically decreasing $H_0(z)$, offering a route to accommodate the Hubble tension.

Load-bearing premise

The analysis assumes the decreasing $H_0(z)$ trend in the 20-bin Master SNe Ia sample is a genuine dynamical signal rather than an artifact of selection biases or the statistical binning procedure.

Editorial extensions

If this is right

  • If the central claim holds, the decreasing $H_0(z)$ seen in binned SNe Ia can be read as a dynamical signature of dark energy–matter interaction rather than a sign of early-universe new physics.
  • The pure evolutionary dark energy model, despite being favored by DESI-style BAO analyses, is the wrong late-universe description for the binned $H_0$ trend; only with interaction does the model reproduce the data.
  • The phantom value $w_{\mathrm{de}} \approx -1.007$ required for the match implies that, under this model, dark energy is mildly phantom, a prediction that can be tested with independent probes of the dark energy equation of state.
  • The DE-DM model offers a concrete alternative to $f(R)$ gravity for the same monotonically decreasing $H_0(z)$, and it does so while keeping the matter term dominant in the late-universe dynamics.
  • Because $w_{\mathrm{de}}$ has a flat posterior in the DE-DM model, the shape of $H_0(z)$ fixes this parameter only through the power-law anchor, meaning the model's predictive power for the equation of state is limited.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the decreasing $H_0(z)$ trend turns out to be a selection-bias artifact, the DE-DM model's match would instead be a physically motivated re-description of that bias; re-running the same analysis on unbinned or bias-corrected SNe Ia would settle which interpretation is right.
  • The flat posterior for $w_{\mathrm{de}}$ suggests a degeneracy direction in the DE-DM dynamics; a joint fit to unbinned distance moduli, not binned $H_0(z)$, could break that degeneracy and tell whether $w_{\mathrm{de}}$ is truly phantom or simply unconstrained.
  • The same interaction mechanism should leave imprints on structure growth and on the matter power spectrum; predictions from the DE-DM model for redshift-space distortions or weak-lensing data would provide independent tests beyond the $H_0(z)$ diagnostic.
  • The model's $H_0(z)$ prediction can be extrapolated to redshifts beyond the sample's last bin; checking it against high-redshift tracers such as BAO or cosmic chronometers at $z > 1.5$ would test whether the declining trend continues or turns over.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

4 major / 5 minor

Summary. The paper studies two late-universe models for the effective running Hubble constant H0(z): a pure evolutionary dark-energy model (DE) in which dark energy is created by the gravitational field, and an interacting model (DE-DM) in which dark energy and matter exchange energy through conservation of their combined energy-momentum tensor. Both models are fitted to the 20-bin Master sample of Type Ia supernovae using an MCMC analysis, and the resulting H0(z) reconstructions are compared with a power-law (PL) reference profile. The paper reports that the DE model is strongly disfavored relative to PL (ΔBIC = 6.6), while for the DE-DM model the dark-energy equation-of-state parameter wde is unconstrained; the authors then fix wde = -1.0073 by minimizing residuals against 100 points drawn from the PL best fit and present the resulting reconstruction as reproducing the power-law decay.

Significance. If the central claim were sound, the paper would be relevant to the Hubble tension by suggesting that dark energy-matter interaction can naturally produce the decreasing H0(z) trend seen in binned supernova data. The theoretical setup in Section 2 is clearly written, the analytic solutions for Ωde(z) are useful, and the authors use standard MCMC software and explicitly acknowledge in the introduction that the power-law trend could be due to selection biases. However, the paper's headline claim is not supported by the reported analysis: the DE-DM model is not actually compared with the data in a model-selection sense, and the key parameter wde is calibrated to the very same power-law profile that the model is then said to reproduce. Because the load-bearing comparison is circular and no DE-DM statistic is reported, the significance of the paper's main conclusion cannot be evaluated from the present manuscript.

major comments (4)
  1. [Abstract and Section 4, Table 1] The claim that the MCMC analysis leads to a 'clear preference of data' for the DE-DM model is not supported by the reported statistics. Table 1 reports no posterior constraint on wde for DE-DM, and the only model-selection quantity in Section 4 is ΔBIC = 6.6 for the DE model, which disfavors that model relative to PL. No ΔBIC, χ², or evidence value is quoted for DE-DM against either PL or ΛCDM. Without such a statistic, the preference asserted in the abstract is a qualitative judgment rather than a result of the comparison procedure.
  2. [Section 4, paragraph after Table 1; Eq. (20)] The procedure used to fix wde is circular. The paper states that wde is unconstrained (flat posterior), then fixes it to wde = -1.0073 by minimizing residuals against 100 points extracted from the power-law best fit to the same Master bin data, and then shows in Eq. (20) and Figure 2 that the DE-DM curve reproduces that power law. Because the PL curve is used both as the target for setting the free parameter and as the reference for the claimed agreement, the match is constructed rather than tested. A valid test would calibrate wde from external data, use an independent prior, or demonstrate with a posterior predictive check that the agreement is not trivially achievable.
  3. [Section 1 and Section 3] The physical interpretation depends on the power-law decay of H0(z) being a genuine dynamical signal. The paper itself notes in Section 1 that the behavior 'could also account for selection biases.' The analysis in Section 3 adopts the 20-bin Master sample and the PL fit as the benchmark without quantifying the impact of selection effects, alternative binning, or distance-modulus systematics. Unless the trend is shown to be astrophysical rather than a statistical artifact, the DE-DM model's ability to mimic that trend carries no cosmological meaning.
  4. [Section 2, Eqs. (5)-(9); Section 4] The conclusions depend on two parameters that are fixed rather than fitted: α = 1 is adopted as 'the simplest case' and Γbar = 0.5 as a 'reference value.' The reported preference of DE-DM could therefore be an artifact of these choices. The analysis should either marginalize over α and Γbar or show that the circular comparison is robust to their variation.
minor comments (5)
  1. [Abstract] The phrase 'phantom matter equation of state parameter' is inaccurate: wde is the dark-energy equation-of-state parameter, not the matter equation of state, and the body of the paper consistently refers to it as the dark energy parameter.
  2. [Section 3] The paper states that a preliminary version of the analysis code will be released in a forthcoming work; to make the MCMC results reproducible, the code or a repository should be provided with the submission.
  3. [Section 4, Table 1] The dash for wde in the DE-DM row should be accompanied by an explicit statement that the parameter is unconstrained by the MCMC, and the table should also list the fixed value wde = -1.0073 used in Eq. (20) with a note explaining its origin.
  4. [Figure 2] The reconstruction of the DE-DM model is shown without uncertainty bands, so the visual agreement with the PL curve cannot be assessed statistically; the paper should show the propagated uncertainty on the fixed-wde reconstruction.
  5. [Section 3, BIC definition] The reference given for the Bayesian Information Criterion is a paper on p-values; please cite the original Schwarz criterion (Schwarz 1978) or a standard textbook in addition to the Jeffreys'-scale references.

Circularity Check

1 steps flagged · score 8.0 of 10

The DE-DM model's reproduction of the power-law H0(z) is manufactured by fitting wde to that same power-law curve; the claimed preference for DE-DM is therefore not an independent data-driven result.

  1. fitted input called prediction [Section 4 (Results), paragraph after Table 1 and Eqs. (19)-(20); echoed in Abstract and Section 5 Conclusions.]
    "In our case, we fix its value by imposing the significant requirement that our Hubble parameter provides a statistically meaningful representation of the power-law discussed in [69, 70]. To this end, we extract from the PL profile, reconstructed by the best-fit values recorded above, 100 points used to minimize the residuals of the two curves (resulting in residuals less than 0.15%). As a result of this procedure, we determine the value of wde = −1.0073, outlining a weak phantom nature of the dark energy."

    In the DE-DM model, wde is the parameter that controls the shape of H0(z) through Eq. (18). The MCMC leaves it unconstrained (flat posterior, Table 1), so the paper fixes it by minimizing residuals against 100 points drawn from the PL best fit of the same binned Master sample. The later conclusion that the model 'can be used to constraint the H0(z) to be a very good representation of the power-law decay observed in [69]' is thus a restatement of the calibration step: the target PL curve is the input used to set the parameter, not an independent prediction. The abstract concedes this ('being left free by data (it has a flat posterior), it is fixed in order to reproduce the decreasing power-law behavior'). The claimed very good representation is forced by construction.

full rationale

The central quantitative result of the paper — that the DE-DM model reproduces the decreasing PL behavior of the running Hubble constant — reduces to a fit: wde is unconstrained by the MCMC and is set by minimizing residuals to the same PL curve that the analysis then claims the model represents. No model-selection statistic is reported for DE-DM (only ΔBIC = 6.6 for DE, which is strongly disfavored relative to PL), so the abstract's 'clear preference of data for the DE-DM interaction model' is not a tested comparison outcome. The PL benchmark itself comes from the authors' own prior works ([69,70], with overlapping authorship), making the calibration anchor self-referential; the introduction even notes the trend 'could also account for selection biases.' However, the decisive circularity is the direct fitting of the free parameter to the target curve, which makes the headline 'representation of the power-law decay' true by construction. This warrants a high circularity score, though the model's H0 and Ωm0 are otherwise fit to external data.

Assumptions & free parameters 6 free parameters · 6 assumptions · 0 invented entities

The central claim rests on several free parameters, including one that is explicitly tuned to match the target power-law trend. The model also relies on an ad hoc creation-rate ansatz and an ad hoc interaction postulate. No new fundamental entity, such as a particle or force, is introduced, so the invented-entities ledger is empty. The heavy reliance on hand-chosen reference values and on a parameter fitted to the benchmark weakens the independent content of the result.

free parameters (6)
  • H0 = 69.872 (DE), 69.959 (DE-DM) km/s/Mpc
    Global expansion-rate normalization fitted to the binned Master sample via MCMC.
  • Omega_m0 = 0.3246 (DE), 0.3084 (DE-DM)
    Present-day matter density parameter fitted to the binned data.
  • wde (DE model) = -1.052 +/- 0.058
    Dark energy equation of state parameter constrained by MCMC in the non-interacting model.
  • wde (DE-DM model) = -1.0073 (fixed by matching PL profile, not constrained by SNe data)
    Data give a flat posterior; the value is chosen by minimizing residuals against 100 points sampled from the power-law fit to the same Master sample.
  • Gamma_bar = 0.5 (chosen by hand)
    Reference value set to preserve the sign of the effective dark energy equation of state today; not fitted to data.
  • alpha = 1 (chosen by hand)
    Simplification adopted because H(z) is weakly sensitive to alpha for z > 1; not fitted.
assumptions (6)
  • domain assumption The universe is described by a flat, isotropic FLRW metric (Equation 1).
    Standard cosmological background assumption used throughout Section 2.
  • domain assumption Radiation energy density is neglected.
    Stated in Section 2 as a simplification, justified for the late-universe redshift range considered.
  • ad hoc to paper The dark energy particle creation rate has the form Gamma = Gamma* H rho_de^{-alpha} (Equation 5).
    This phenomenological ansatz is introduced as a mixed version of earlier rates and has no independent derivation.
  • ad hoc to paper Dark energy and matter interact via conservation of the sum of their energy-momentum tensors (Equation 13).
    The interaction is postulated rather than derived from a Lagrangian or microphysical model.
  • ad hoc to paper The reference values Gamma_bar = 0.5 and alpha = 1 are adopted.
    Chosen by hand for simplicity and comparability, not determined by the data analysis.
  • domain assumption The binned Master sample and its power-law fit are valid observational benchmarks.
    The dataset and PL reference are taken from prior work [69,70]; the paper does not independently validate the binning or the absence of selection biases.

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Cite this review

Pith. "Pith review of Two Dynamical Scenarios for Binned Master Sample Interpretation." pith.science (2026). https://pith.science/paper/P3YSLBYQ

@misc{pith2026250714048,
  author       = {Pith},
  title        = {Pith review of: Two Dynamical Scenarios for Binned Master Sample Interpretation},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/P3YSLBYQ}},
  note         = {Machine review of arXiv:2507.14048}
}
abstract

We analyze two different scenarios for the late Universe dynamics, resulting into Hubble parameters deviating from the $\Lambda$CDM, mainly for the presence of an additional free parameter, which is the dark energy parameter. The first model consists of a pure evolutionary dark energy paradigm, as result of its creation by the gravitational field of the expanding Universe. The second model also considers an interaction of the evolutionary dark energy with the matter component, postulated via the conservation of the sum of their ideal energy-momentum tensors. These two models are then compared \textit{via} the diagnostic tool of the effective running Hubble constant, with the binned data of the so-called ``Master sample'' for the Type Ia Supernovae. The comparison procedures, based on a standard MCMC analysis, led to a clear preference of data for the dark energy - matter interaction model, which is associated to a phantom matter equation of state parameter (very close to $-1$) when, being left free by data (it has a flat posterior), it is fixed in order to reproduce the decreasing power-law behavior of the effective running Hubble constant, already discussed in literature.

Figures

Figures reproduced from arXiv: 2507.14048 by the authors.

Figure 1
Figure 1. One-dimensional posterior probability distributions and two-dimensional [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Reconstruction of the effective running Hubble constant for the DE model, DE-DM [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. BAO miscalibration cannot rescue late-time solutions to the Hubble tension

    astro-ph.CO 2025-10 accept novelty 6.0 of 10

    Even after rescaling BAO data to prefer H0≈73 km/s/Mpc, none of six tested late-time dark-energy models can resolve the Hubble tension once unanchored SNeIa and CMB geometry are included.

Reference graph

Works this paper leans on

120 extracted references · 15 canonical work pages · cited by 1 Pith paper

  1. [1]

    A flat Universe from high-resolution maps of the cosmic microwave background radiation

    P. de Bernardis et al. “A flat Universe from high-resolution maps of the cosmic microwave background radiation”. In: Nature 404.6781 (Apr. 2000), pp. 955–959. doi: 10 . 1038 / 35010035. arXiv: astro-ph/0004404 [astro-ph]

    arXiv 2000

  2. [2]

    Nine-year Wilkinson Microwave Anisotropy Probe (WMAP) Ob- servations: Final Maps and Results

    C. L. Bennett et al. “Nine-year Wilkinson Microwave Anisotropy Probe (WMAP) Ob- servations: Final Maps and Results”. In:ApJ S.R. 208.2, 20 (Oct. 2013), p. 20. doi: 10.1088/0067-0049/208/2/20. arXiv: 1212.5225 [astro-ph.CO]

    arXiv 2013

  3. [3]

    A comprehensive measurement of the local value of the Hubble constant with 1 km s−1 Mpc−1 uncertainty from the Hubble Space Telescope and the SH0ES team

    Adam G Riess et al. “A comprehensive measurement of the local value of the Hubble constant with 1 km s−1 Mpc−1 uncertainty from the Hubble Space Telescope and the SH0ES team”. In:The Astrophysical journal letters934.1 (2022), p. L7.doi: 10.3847/ 2041-8213/ac5c5b

    2022

  4. [4]

    Planck 2018 results-VI. Cosmological parameters

    Nabila Aghanim et al. “Planck 2018 results-VI. Cosmological parameters”. In:Astronomy & Astrophysics641 (2020), A6. 8

    2020

  5. [5]

    The CosmoVerse White Paper: Addressing observational tensions in cosmology with systematics and fundamental physics

    Eleonora Di Valentino et al. “The CosmoVerse White Paper: Addressing observational tensions in cosmology with systematics and fundamental physics”. In:Phys. Dark Univ. (2025), pp. 1–416

    2025

  6. [6]

    In the realm of the Hubble tension—a review of solutions

    Eleonora Di Valentino et al. “In the realm of the Hubble tension—a review of solutions”. In: Classical and Quantum Gravity38.15 (July 2021), p. 153001.doi: 10.1088/1361- 6382/ac086d

    doi:10.1088/1361- 2021

  7. [7]

    Seven hints that early-time new physics alone is not sufficient to solve the Hubble tension

    Sunny Vagnozzi. “Seven hints that early-time new physics alone is not sufficient to solve the Hubble tension”. In:Universe 9.9 (2023), p. 393

    2023

  8. [8]

    Exploring the Hubble tension with a late time Modified Gravity scenario

    Luis A. Escamilla et al. “Exploring the Hubble tension with a late time Modified Gravity scenario”.In: Phys. Dark Univ.46(2024),p.101652. doi: 10.1016/j.dark.2024.101652. arXiv: 2408.04354 [astro-ph.CO]

    arXiv 2024

Show all 120 references
  1. [9]

    Kinetic model for dark energy—dark matter interaction: Sce- nario for the hubble tension

    Giovanni Montani et al. “Kinetic model for dark energy—dark matter interaction: Sce- nario for the hubble tension”. In:Phys. Dark Univ.48 (2025), p. 101848.doi: 10.1016/ j.dark.2025.101848. arXiv: 2404.15977 [gr-qc]

    2025

  2. [10]

    Slow-rolling scalar dynamics as solution for the Hubble tension

    Giovanni Montani, Nakia Carlevaro, and Maria Giovanna Dainotti. “Slow-rolling scalar dynamics as solution for the Hubble tension”. In:Physics of the Dark Universe44 (May 2024), p. 101486.doi: 10.1016/j.dark.2024.101486

    2024

  3. [11]

    Metric f (R) gravity with dynamical dark energy as a scenario for the Hubble tension

    Giovanni Montani et al. “Metric f (R) gravity with dynamical dark energy as a scenario for the Hubble tension”. In:Monthly Notices of the Royal Astronomical Society: Letters 527.1 (Oct. 2023), pp. L156–L161.doi: 10.1093/mnrasl/slad159

    2023 doi

  4. [12]

    f(R) gravity in the Jor- dan frame as a paradigm for the Hubble tension

    Tiziano Schiavone, Giovanni Montani, and Flavio Bombacigno. “f(R) gravity in the Jor- dan frame as a paradigm for the Hubble tension”. In:Monthly Notices of the Royal Astro- nomical Society: Letters522.1(Mar.2023),pp.L72–L77. doi: 10.1093/mnrasl/slad041

    2023 doi

  5. [13]

    Running Hubble constant from the SNe Ia Pantheon sample?

    Tiziano Schiavone et al. “Running Hubble constant from the SNe Ia Pantheon sample?” In: 17th Italian-Korean Symposium on Relativistic Astrophysics. May 2022. arXiv:2205. 07033 [astro-ph.CO]

    2022

  6. [14]

    Introduction to modified gravity and gravita- tional alternative for dark energy

    Shin’ichi Nojiri and Sergei D. Odintsov. “Introduction to modified gravity and gravita- tional alternative for dark energy”. In:eConf C0602061 (2006). Ed. by Andrzej Borowiec, p. 06. doi: 10.1142/S0219887807001928

    2006 doi

  7. [15]

    New constraints on interacting dark energy from DESI DR2 BAO observations

    Emanuelly Silva et al. “New constraints on interacting dark energy from DESI DR2 BAO observations”. In:Phys. Rev. D111.12, 123511 (June 2025), p. 123511.doi: 10.1103/ qqc6-76z4. arXiv: 2503.23225 [astro-ph.CO]

    2025 arXiv

  8. [16]

    Implications of distance duality violation for theH_0 tension and evolving dark energy

    Elsa M Teixeira et al. “Implications of distance duality violation for theH_0 tension and evolving dark energy”. In:arXiv preprint arXiv:2504.10464(2025)

    2025 arXiv

  9. [17]

    Inflation, the Hubble tension, and early dark energy: An alternative overview

    William Giarè. “Inflation, the Hubble tension, and early dark energy: An alternative overview”. In:Physical Review D109.12 (2024), p. 123545

    2024

  10. [18]

    Small-amplitude Red Giants Elucidate the Nature of the Tip of the Red Giant Branch as a Standard Candle

    Richard I. Anderson, Nolan W. Koblischke, and Laurent Eyer. “Small-amplitude Red Giants Elucidate the Nature of the Tip of the Red Giant Branch as a Standard Candle”. In: ApJ Lett.963.2, L43 (Mar. 2024), p. L43.doi: 10.3847/2041-8213/ad284d. arXiv: 2303.04790 [astro-ph.CO]

    2024 arXiv

  11. [19]

    The Pantheon+ Analysis: The Full Data Set and Light-curve Release

    Dan Scolnic et al. “The Pantheon+ Analysis: The Full Data Set and Light-curve Release”. In: The Astrophysical Journal 938.2 (Oct. 2022), p. 113. doi: 10 . 3847 / 1538 - 4357 / ac8b7a

    2022

  12. [20]

    The Complete Light-curve Sample of Spectroscopically Confirmed SNe Ia from Pan-STARRS1 and Cosmological Constraints from the Combined Pantheon Sample

    D. M. Scolnic et al. “The Complete Light-curve Sample of Spectroscopically Confirmed SNe Ia from Pan-STARRS1 and Cosmological Constraints from the Combined Pantheon Sample”. In: ApJ 859.2, 101 (June 2018), p. 101.doi: 10.3847/1538- 4357/aab9bb . arXiv: 1710.00845 [astro-ph.CO]. 9

    2018 arXiv

  13. [21]

    The Pantheon+ Analysis: Cosmological Constraints

    Dillon Brout et al. “The Pantheon+ Analysis: Cosmological Constraints”. In:ApJ 938.2 (2022), p. 110.doi: 10.3847/1538-4357/ac8e04. arXiv: 2202.04077 [astro-ph.CO]

    2022 arXiv

  14. [22]

    CATS: The Hubble Constant from Standardized TRGB and Type Ia Supernova Measurements

    D. Scolnic et al. “CATS: The Hubble Constant from Standardized TRGB and Type Ia Supernova Measurements”. In:Astrophys. J. Lett.954.1 (2023), p. L31.doi: 10.3847/ 2041-8213/ace978. arXiv: 2304.06693 [astro-ph.CO]

    2023 arXiv

  15. [23]

    Cosmological Results from the RAISIN Survey: Using Type Ia Su- pernovae in the Near Infrared as a Novel Path to Measure the Dark Energy Equation of State

    D. O. Jones et al. “Cosmological Results from the RAISIN Survey: Using Type Ia Su- pernovae in the Near Infrared as a Novel Path to Measure the Dark Energy Equation of State”. In:Astrophys. J.933.2 (2022), p. 172.doi: 10.3847/1538-4357/ac755b. arXiv: 2201.07801 [astro-ph.CO]

    2022 arXiv

  16. [24]

    Comparing Tip of the Red Giant Branch Distance Scales: An Independent Reduction of the Carnegie-Chicago Hubble Program and the Value of the Hubble Constant

    Gagandeep S. Anand et al. “Comparing Tip of the Red Giant Branch Distance Scales: An Independent Reduction of the Carnegie-Chicago Hubble Program and the Value of the Hubble Constant”. In:Astrophys. J.932.1 (2022), p. 15.doi: 10.3847/1538-4357/ ac68df. arXiv: 2108.00007 [astro-ph.CO]

    2022 arXiv

  17. [26]

    Carnegie Supernova Project-I and -II: Measurements ofH0 using Cepheid,TRGB,andSBFDistanceCalibrationtoTypeIaSupernovae

    Syed A. Uddin et al. “Carnegie Supernova Project-I and -II: Measurements ofH0 using Cepheid,TRGB,andSBFDistanceCalibrationtoTypeIaSupernovae”.In: arXiv:2308.01875 (Aug. 2023). arXiv:2308.01875 [astro-ph.CO]

    2023 arXiv

  18. [27]

    The Mira Distance to M101 and a 4% Measurement of H0

    Caroline D. Huang et al. “The Mira Distance to M101 and a 4% Measurement of H0”. In: Astrophys. J.963.2 (2024), p. 83.doi: 10.3847/1538-4357/ad1ff8. arXiv: 2312.08423 [astro-ph.CO]

    2024 arXiv

  19. [28]

    Reconnaissance with JWST of the J-region Asymptotic Giant Branch in Distance Ladder Galaxies: From Irregular Luminosity Functions to Approximation of the Hubble Constant

    Siyang Li et al. “Reconnaissance with JWST of the J-region Asymptotic Giant Branch in Distance Ladder Galaxies: From Irregular Luminosity Functions to Approximation of the Hubble Constant”. In:Astrophys. J. 966.1 (2024), p. 20. doi: 10 . 3847 / 1538 - 4357/ad2f2b. arXiv: 2401....

    2024 arXiv

  20. [29]

    Cosmicflows-4:TheCalibrationofOpticalandInfraredTully–Fisher Relations

    EhsanKourkchietal.“Cosmicflows-4:TheCalibrationofOpticalandInfraredTully–Fisher Relations”. In:Astrophys. J.896.1 (2020), p. 3.doi: 10.3847/1538-4357/ab901c. arXiv: 2004.14499 [astro-ph.GA]

    2020 arXiv

  21. [30]

    Using the Baryonic Tully–Fisher Relation to Measure H o

    James Schombert, Stacy McGaugh, and Federico Lelli. “Using the Baryonic Tully–Fisher Relation to Measure H o”. In: Astron. J. 160.2 (2020), p. 71. doi: 10 . 3847 / 1538 - 3881/ab9d88. arXiv: 2006.08615 [astro-ph.CO]

    2020 arXiv

  22. [31]

    Leveraging SN Ia spectroscopic similarity to improve the measurement of H0

    Yukei S. Murakami et al. “Leveraging SN Ia spectroscopic similarity to improve the measurement of H0”. In:JCAP 11 (2023), p. 046.doi: 10.1088/1475-7516/2023/11/

    2023 doi

  23. [32]

    Small Magellanic Cloud Cepheids Observed with the Hubble Space Telescope Provide a New Anchor for the SH0ES Distance Ladder

    Louise Breuval et al. “Small Magellanic Cloud Cepheids Observed with the Hubble Space Telescope Provide a New Anchor for the SH0ES Distance Ladder”. In:arXiv:2404.08038 (Apr. 2024). arXiv:2404.08038 [astro-ph.CO]

    2024 arXiv

  24. [33]

    Measurement of the CMB temperature power spectrum and con- straints on cosmology from the SPT-3G 2018 TT, TE, and EE dataset

    L. Balkenhol et al. “Measurement of the CMB temperature power spectrum and con- straints on cosmology from the SPT-3G 2018 TT, TE, and EE dataset”. In:Phys. Rev. D 108.2 (2023), p. 023510. doi: 10.1103/PhysRevD.108.023510 . arXiv: 2212.05642 [astro-ph.CO]

    2023 arXiv

  25. [34]

    The Atacama Cosmology Telescope: DR4 Maps and Cosmological Parameters

    Simone Aiola et al. “The Atacama Cosmology Telescope: DR4 Maps and Cosmological Parameters”. In: JCAP 12 (2020), p. 047. doi: 10 . 1088 / 1475 - 7516 / 2020 / 12 / 047. arXiv: 2007.07288 [astro-ph.CO]

    2020 arXiv

  26. [35]

    A proposal to improve the accuracy of cosmolog- ical observables and address the Hubble tension problem

    Horst Foidl and Tanja Rindler-Daller. “A proposal to improve the accuracy of cosmolog- ical observables and address the Hubble tension problem”. In:A& A 686, A210 (2024), A210. doi: 10.1051/0004-6361/202348955. 10

    2024 doi

  27. [36]

    DeterminingH0 from distance sum rule combining gamma-ray bursts with observational Hubble data and strong gravitational lensing

    Orlando Luongo and Marco Muccino. “DeterminingH0 from distance sum rule combining gamma-ray bursts with observational Hubble data and strong gravitational lensing”. In: arXiv e-prints, arXiv:2412.18493 (Dec. 2024), arXiv:2412.18493.doi: 10.48550/arXiv. 2412.18493. arXiv: 2412....

    2024 doi

  28. [37]

    Deep Learning Based Recalibration of SDSS and DESI BAO Al- leviates Hubble and Clustering Tensions

    Rahul Shah et al. “Deep Learning Based Recalibration of SDSS and DESI BAO Al- leviates Hubble and Clustering Tensions”. In: arXiv e-prints, arXiv:2412.14750 (Dec. 2024), arXiv:2412.14750. doi: 10 . 48550 / arXiv . 2412 . 14750. arXiv: 2412 . 14750 [astro-ph.CO]

    2024 doi arXiv

  29. [38]

    Tensions between the early and late Universe

    Licia Verde, Tommaso Treu, and Adam G. Riess. “Tensions between the early and late Universe”. In: Nature Astronomy 3.10 (Sept. 2019), pp. 891–895.issn: 2397-3366. doi: 10.1038/s41550-019-0902-0. url: http://dx.doi.org/10.1038/s41550-019-0902- 0

    2019 doi

  30. [39]

    The Carnegie-Chicago Hubble Program. VIII. An Inde- pendent Determination of the Hubble Constant Based on the Tip of the Red Giant Branch*

    Wendy L. Freedman et al. “The Carnegie-Chicago Hubble Program. VIII. An Inde- pendent Determination of the Hubble Constant Based on the Tip of the Red Giant Branch*”. In:The Astrophysical Journal882.1 (Aug. 2019), p. 34.issn: 1538-4357. doi: 10.3847/1538-4357/ab2f73. url: http...

    2019 doi

  31. [40]

    Calibration of the Tip of the Red Giant Branch (TRGB)

    Wendy L. Freedman et al. “Calibration of the Tip of the Red Giant Branch (TRGB)”. In: (Feb. 2020).doi: 10.3847/1538-4357/ab7339. arXiv: 2002.01550 [astro-ph.GA]

    2020 arXiv

  32. [41]

    The Parallax ofω Centauri Mea- sured from Gaia EDR3 and a Direct, Geometric Calibration of the Tip of the Red Gi- ant Branch and the Hubble Constant

    John Soltis, Stefano Casertano, and Adam G. Riess. “The Parallax ofω Centauri Mea- sured from Gaia EDR3 and a Direct, Geometric Calibration of the Tip of the Red Gi- ant Branch and the Hubble Constant”. In:Astrophys. J. Lett.908.1 (2021), p. L5.doi: 10.3847/2041-8213/abdbad. a...

    2021 arXiv

  33. [42]

    Analysing the large-scale bulk flow using cosmicflows4: increasing tension with the standard cosmological model

    Richard Watkins et al. “Analysing the large-scale bulk flow using cosmicflows4: increasing tension with the standard cosmological model”. In:Monthly Notices of the Royal Astro- nomical Society 524.2 (Sept. 2023), pp. 1885–1892. doi: 10 . 1093 / mnras / stad1984. arXiv: 2302.02...

    2023 arXiv

  34. [43]

    Exploring the evi- dence for a large local void with supernovae Ia data

    Vladimir V. Luković, Balakrishna S. Haridasu, and Nicola Vittorio. “Exploring the evi- dence for a large local void with supernovae Ia data”. In:Monthly Notices of the Royal Astronomical Society491.2 (Jan. 2020), pp. 2075–2087.doi: 10.1093/mnras/stz3070. arXiv: 1907.11219 [ast...

    2020 arXiv

  35. [44]

    New constraint of the Hubble constant by proper motions of radio components observed in AGN twin-jets

    Wei-Jian Lu and Yi-Ping Qin. “New constraint of the Hubble constant by proper motions of radio components observed in AGN twin-jets”. In:Research in Astronomy and Astro- physics 21.10 (Nov. 2021), p. 261.issn: 1674-4527.doi: 10.1088/1674-4527/21/10/261. url: http://dx.doi.org/...

    2021 doi

  36. [45]

    Unbiased likelihood-free infer- enceoftheHubbleconstantfromlightstandardsirens

    Francesca Gerardi, Stephen M. Feeney, and Justin Alsing. “Unbiased likelihood-free infer- enceoftheHubbleconstantfromlightstandardsirens”.In: arXiv e-prints,arXiv:2104.02728 (Apr. 2021), arXiv:2104.02728. arXiv:2104.02728 [astro-ph.CO]

    2021 arXiv

  37. [46]

    arXiv: 2306.00070 [astro-ph.CO]

    arXiv

  38. [47]

    Rachel Gray, Chris Messenger, and John Veitch.A Pixelated Approach to Galaxy Cat- alogue Incompleteness: Improving the Dark Siren Measurement of the Hubble Constant

  39. [48]

    arXiv: 2110.11731 [astro-ph.CO]

    Simone Mozzon et al.Does non-stationary noise in LIGO and Virgo affect the estimation of H0? 2021. arXiv: 2110.11731 [astro-ph.CO]. 11

    2021 arXiv

  40. [50]

    Forecast of Observing Time Delay of Strongly Lensed Quasars with the Muztagh-Ata 1.93 m Telescope

    Shanhao Zhu et al. “Forecast of Observing Time Delay of Strongly Lensed Quasars with the Muztagh-Ata 1.93 m Telescope”. In:Research in Astronomy and Astrophysics23.3, 035001 (Mar. 2023), p. 035001.doi: 10.1088/1674-4527/acaf4e . arXiv: 2203.15680 [astro-ph.CO]

    2023 arXiv

  41. [51]

    A standard siren measurement of the Hubble constant using gravitational wave events from the first three LIGO/Virgo observing runs and the DESI Legacy Survey

    Antonella Palmese et al. A standard siren measurement of the Hubble constant using gravitational wave events from the first three LIGO/Virgo observing runs and the DESI Legacy Survey. 2021. arXiv:2111.06445 [astro-ph.CO]

    2021 arXiv

  42. [52]

    A 5 per cent measurement of the Hubble-Lemaıˆtre constant from Type II supernovae

    T. de Jaeger et al. “A 5 per cent measurement of the Hubble-Lemaıˆtre constant from Type II supernovae”. In:Monthly Notices of the Royal Astronomical Society514.3 (Aug. 2022),pp.4620–4628. doi: 10.1093/mnras/stac1661.arXiv: 2203.08974 [astro-ph.CO]

    2022 arXiv

  43. [53]

    Assessing the effect of mass-model assumptions on measuring the Hubble constant from the cluster-lensed supernova Refsdal

    Yuting Liu and Masamune Oguri. “Assessing the effect of mass-model assumptions on measuring the Hubble constant from the cluster-lensed supernova Refsdal”. In:Phys. Rev. D 111.12(2025),p.123506. doi: 10.1103/v857-ylw5.arXiv: 2402.13476 [astro-ph.CO]

    2025 arXiv

  44. [54]

    The Hubble Constant from Infrared Surface Brightness Fluc- tuation Distances*

    John P. Blakeslee et al. “The Hubble Constant from Infrared Surface Brightness Fluc- tuation Distances*”. In:The Astrophysical Journal911.1 (Apr. 2021), p. 65.issn: 1538-

    2021

  45. [55]

    TheMegamaserCosmologyProject.XIII.CombinedHubbleConstant Constraints

    D.W.Pesceetal.“TheMegamaserCosmologyProject.XIII.CombinedHubbleConstant Constraints”. In:The Astrophysical Journal Letters891.1 (Feb. 2020), p. L1.issn: 2041-

    2020

  46. [56]

    DESI DR2 Results II: Measurements of Baryon Acoustic Oscil- lations and Cosmological Constraints

    M. Abdul-Karim et al. “DESI DR2 Results II: Measurements of Baryon Acoustic Oscil- lations and Cosmological Constraints”. In: (2025). arXiv:2503.14738 [astro-ph.CO] . url: https://arxiv.org/abs/2503.14738

    2025 arXiv

  47. [57]

    Accelerating universes with scaling dark matter

    Michel Chevallier and David Polarski. “Accelerating universes with scaling dark matter”. In: International Journal of Modern Physics D10.02 (2001), pp. 213–223

    2001

  48. [58]

    Exploring the expansion history of the universe

    Eric V Linder. “Exploring the expansion history of the universe”. In: Physical review letters 90.9 (2003), p. 091301

    2003

  49. [59]

    DESI 2024 VI: cosmological constraints from the measurements of baryon acoustic oscillations

    A. G. Adame et al. “DESI 2024 VI: cosmological constraints from the measurements of baryon acoustic oscillations”. In:JCAP 02 (2025), p. 021. doi: 10.1088/1475- 7516/ 2025/02/021. arXiv: 2404.03002 [astro-ph.CO]

    2025 arXiv

  50. [60]

    An overview of what current data can (and cannot yet) say about evolving dark energy

    William Giarè et al. “An overview of what current data can (and cannot yet) say about evolving dark energy”. In:Physics of the Dark Universe(2025), p. 101906

    2025

  51. [61]

    Dynamical Dark Energy Beyond Planck? Constraints from multiple CMB probes, DESI BAO and Type-Ia Supernovae

    William Giarè. “Dynamical Dark Energy Beyond Planck? Constraints from multiple CMB probes, DESI BAO and Type-Ia Supernovae”. In:arXiv preprint arXiv:2409.17074 (2024)

    2024 arXiv

  52. [63]

    Extended Dark Energy analysis using DESI DR2 BAO measurements

    K Lodha et al. “Extended Dark Energy analysis using DESI DR2 BAO measurements”. In: arXiv preprint arXiv:2503.14743(2025)

    2025 arXiv

  53. [64]

    Phenomenology of Λ-CDM Model: A Possibility of Accelerating Uni- verse with Positive Pressure

    Saibal Ray et al. “Phenomenology of Λ-CDM Model: A Possibility of Accelerating Uni- verse with Positive Pressure”. In:International Journal of Theoretical Physics50.3 (Mar. 2011), pp. 939–951.doi: 10.1007/s10773-010-0639-0. arXiv: 0711.0686 [gr-qc]. 12

    2011 arXiv

  54. [65]

    Decay of Cosmological Constant as Bose Con- densate Evaporation

    Irina Dymnikova and Maxim Khlopov. “Decay of Cosmological Constant as Bose Con- densate Evaporation”. In:Modern Physics Letters A15.38-39 (Jan. 2000), pp. 2305–2314. doi: 10.1142/S0217732300002966. arXiv: astro-ph/0102094 [astro-ph]

    arXiv

  55. [66]

    Formation of structure in a universe with unstable neutrinos

    A. G. Doroshkevich and M. Iu. Khlopov. “Formation of structure in a universe with unstable neutrinos”. In:Mon. Not. RAS 211 (Nov. 1984), pp. 277–282.doi: 10.1093/ mnras/211.2.277

    1984

  56. [67]

    DoesDESI2024Confirm ΛCDM?

    EoinÓColgáinetal.“DoesDESI2024Confirm ΛCDM?” In:arXiv preprint arXiv:2404.08633 (2024)

    2024 arXiv

  57. [68]

    On the evolution of the Hubble constant with the SNe Ia pantheon sample and baryon acoustic oscillations: a feasibility study for GRB-cosmology in 2030

    Maria Giovanna Dainotti et al. “On the evolution of the Hubble constant with the SNe Ia pantheon sample and baryon acoustic oscillations: a feasibility study for GRB-cosmology in 2030”. In:Galaxies 10.1 (2022), p. 24

    2022

  58. [69]

    M. G. Dainotti et al. A New Master Supernovae Ia sample and the investigation of the H0 tension. 2025. arXiv:2501.11772 [astro-ph.CO]. url: https://arxiv.org/abs/ 2501.11772

    2025 arXiv

  59. [70]

    The effective running Hubble constant in SNe Ia as a marker for the dark energy nature

    E. Fazzari et al. “The effective running Hubble constant in SNe Ia as a marker for the dark energy nature”. In: (June 2025). arXiv:2506.04162 [astro-ph.CO]

    2025

  60. [71]

    On the Hubble constant tension in the SNe Ia Pantheon sample

    Maria Giovanna Dainotti et al. “On the Hubble constant tension in the SNe Ia Pantheon sample”. In:The Astrophysical Journal912.2 (2021), p. 150

    2021

  61. [72]

    On the statistical assumption on the distance moduli of Supernovae Ia and its impact on the determination of cosmological parameters

    M. G. Dainotti et al. “On the statistical assumption on the distance moduli of Supernovae Ia and its impact on the determination of cosmological parameters”. In:JHEAp 41 (2024), pp. 30–41. doi: 10.1016/j.jheap.2024.01.001

    2024 doi

  62. [73]

    Redshift evolution of the underlying type Ia supernova stretch dis- tribution

    N. Nicolas et al. “Redshift evolution of the underlying type Ia supernova stretch dis- tribution”. In: Astronomy & Astrophysics 649 (May 2021), A74. issn: 1432-0746. doi: 10.1051/0004- 6361/202038447 . url: http://dx.doi.org/10.1051/0004- 6361/ 202038447

    2021 doi

  63. [74]

    Status Report on the Chicago-Carnegie Hubble Program (CCHP): Measurement of the Hubble Constant Using the Hubble and James Webb Space Telescopes

    Wendy L. Freedman et al. “Status Report on the Chicago-Carnegie Hubble Program (CCHP): Measurement of the Hubble Constant Using the Hubble and James Webb Space Telescopes”. In:ApJ 985.2, 203 (June 2025), p. 203.doi: 10.3847/1538-4357/adce78. arXiv: 2408.06153 [astro-ph.CO]

    2025 arXiv

  64. [75]

    Evolution of an effective Hubble constant in f (R) modified gravity

    Tiziano Schiavone and Giovanni Montani. “Evolution of an effective Hubble constant in f (R) modified gravity”. In:arXiv preprint arXiv:2408.01410(2024)

    2024 arXiv

  65. [76]

    Can we learn from matter creation to solve theH0 tension problem?

    Emilio Elizalde, Martiros Khurshudyan, and Sergei D Odintsov. “Can we learn from matter creation to solve theH0 tension problem?” In:The European Physical Journal C 84.8 (2024), p. 782

    2024

  66. [77]

    Investigating f (R)-Inflation: background evolution and constraints

    Elisa Fazzari et al. Investigating f (R)-Inflation: background evolution and constraints

  67. [78]

    Challenging ΛCDM: 5σ Evidence for a Dynamical Dark Energy Late-TimeTransition

    Mateus Scherer et al. “Challenging ΛCDM: 5σ Evidence for a Dynamical Dark Energy Late-TimeTransition”.In: arXiv e-prints,arXiv:2504.20664(Apr.2025),arXiv:2504.20664. doi: 10.48550/arXiv.2504.20664. arXiv: 2504.20664 [astro-ph.CO]

    2025 doi arXiv

  68. [79]

    The gamma-ray bursts fundamental plane correlation as a cos- mological tool

    M. G. Dainotti et al. “The gamma-ray bursts fundamental plane correlation as a cos- mological tool”. In: Mon. Not. Roy. Astron. Soc. 518.2 (2023), pp. 2201–2240. doi: 10.1093/mnras/stac2752. arXiv: 2209.08675 [astro-ph.HE]

    2023 arXiv

  69. [80]

    Influence of particle creation on flat and negative curved FLRW universes

    Giovanni Montani. “Influence of particle creation on flat and negative curved FLRW universes”. In:Classical and Quantum Gravity18.1 (2001), p. 193

    2001

  70. [81]

    A new binning method to choose a standard set of Quasars

    Maria Giovanna Dainotti et al. “A new binning method to choose a standard set of Quasars”. In:Physics of the Dark Universe44 (2024), p. 101428. 13

    2024

  71. [82]

    The evidence for a spatially flat Universe

    George Efstathiou and Steven Gratton. “The evidence for a spatially flat Universe”. In: Monthly Notices of the Royal Astronomical Society: Letters496.1 (2020), pp. L91–L95

    2020

  72. [83]

    Weinberg

    S. Weinberg. Gravitation and Cosmology: Principles and Applications of the General Theory of Relativity. Wiley, 1972.isbn: 9780471925675

    1972

  73. [84]

    On the thermodynamics of matter creation in cosmology

    MO Calvao, JAS Lima, and I Waga. “On the thermodynamics of matter creation in cosmology”. In:Physics Letters A162.3 (1992), pp. 223–226

    1992

  74. [85]

    Coupled quintessence

    Luca Amendola. “Coupled quintessence”. In: Phys. Rev. D 62.4, 043511 (Aug. 2000), p. 043511. doi: 10.1103/PhysRevD.62.043511. arXiv: astro-ph/9908023 [astro-ph]

    2000 arXiv

  75. [86]

    Cosmological evolution with interaction between dark energy and dark matter

    Yuri L. Bolotin et al. “Cosmological evolution with interaction between dark energy and dark matter”. In: International Journal of Modern Physics D 24.03 (Feb. 2015), p. 1530007. issn: 1793-6594. doi: 10.1142/s0218271815300074. url: http://dx.doi. org/10.1142/S0218271815300074

    2015 doi

  76. [87]

    Dark matter and dark energy interactions: theoretical challenges, cos- mological implications and observational signatures

    B Wang et al. “Dark matter and dark energy interactions: theoretical challenges, cos- mological implications and observational signatures”. In:Reports on Progress in Physics 79.9 (Aug. 2016), p. 096901.issn: 1361-6633. doi: 10.1088/0034-4885/79/9/096901 . url: http://dx.doi.or...

    2016 doi

  77. [88]

    Transition of the dark energy equation of state in an interacting holographic dark energy model

    Bin Wang, Yungui Gong, and Elcio Abdalla. “Transition of the dark energy equation of state in an interacting holographic dark energy model”. In:Physics Letters B 624.3–4 (Sept. 2005), pp. 141–146.issn: 0370-2693. doi: 10.1016/j.physletb.2005.08.008 . url: http://dx.doi.org/10....

    2005 doi

  78. [89]

    Phantom behavior via cosmological creation of par- ticles

    Rafael C Nunes and Diego Pavón. “Phantom behavior via cosmological creation of par- ticles”. In:Physical Review D91.6 (2015), p. 063526

    2015

  79. [90]

    Acosmographicanalysis ofholographic darken- ergymodels

    Supriya Panand Subenoy Chakraborty. “Acosmographicanalysis ofholographic darken- ergymodels”.In: International Journal of Modern Physics D23.11(Oct.2014),p.1450092. issn: 1793-6594. doi: 10.1142/s0218271814500928 . url: http://dx.doi.org/10. 1142/S0218271814500928

    2014 doi

  80. [91]

    Cosmologies with energy exchange

    John D. Barrow and T. Clifton. “Cosmologies with energy exchange”. In:Physical Review D 73.10 (May 2006).issn: 1550-2368. doi: 10.1103/physrevd.73.103520. url: http: //dx.doi.org/10.1103/PhysRevD.73.103520

    2006 doi

  81. [92]

    Consequences of dark matter-dark energy interaction on cosmological parameters derived from SNIa data

    Luca Amendola, Gabriela Camargo Campos, and Rogerio Rosenfeld. “Consequences of dark matter-dark energy interaction on cosmological parameters derived from SNIa data”. In: Phys. Rev. D 75 (2007), p. 083506. doi: 10 . 1103 / PhysRevD . 75 . 083506. arXiv: astro-ph/0610806

    2007 arXiv

  82. [93]

    Effects of the interaction between dark energy and dark matter on cosmological parameters

    Jian-Hua He and Bin Wang. “Effects of the interaction between dark energy and dark matter on cosmological parameters”. In:Journal of Cosmology and Astroparticle Physics 2008.06 (June 2008), p. 010.issn: 1475-7516. doi: 10.1088/1475-7516/2008/06/010 . url: http://dx.doi.org/10....

    2008 doi

  83. [94]

    Superacceleration as the signature of a dark sector interaction

    Subinoy Das, Pier Stefano Corasaniti, and Justin Khoury. “Superacceleration as the signature of a dark sector interaction”. In:Physical Review D 73.8 (Apr. 2006). issn: 1550-2368. doi: 10.1103/physrevd.73.083509 . url: http://dx.doi.org/10.1103/ PhysRevD.73.083509

    2006 doi

  84. [97]

    Observational constraints on an interacting dark energy model

    Jussi Väliviita, Roy Maartens, and Elisabetta Majerotto. “Observational constraints on an interacting dark energy model”. In:Monthly Notices of the Royal Astronomical Society 402.4 (Mar. 2010), pp. 2355–2368.issn: 1365-2966. doi: 10.1111/j.1365-2966.2009. 16115.x. url: http://...

    2010

  85. [98]

    Linear and nonlinear interactions in the dark sector

    Luis P. Chimento. “Linear and nonlinear interactions in the dark sector”. In:Physical Review D 81.4 (Feb. 2010).issn: 1550-2368. doi: 10.1103/physrevd.81.043525. url: http://dx.doi.org/10.1103/PhysRevD.81.043525

    2010 doi

  86. [99]

    Large-scale instability in inter- acting dark energy and dark matter fluids

    Jussi Väliviita, Elisabetta Majerotto, and Roy Maartens. “Large-scale instability in inter- acting dark energy and dark matter fluids”. In:Journal of Cosmology and Astroparticle Physics 2008.07 (July 2008), p. 020.issn: 1475-7516. doi: 10.1088/1475-7516/2008/ 07/020. url: http...

    2008 doi

  87. [100]

    Interacting dark sector with transversal inter- action

    Luis P. Chimento and Martín G. Richarte. “Interacting dark sector with transversal inter- action”. In:AIP Conference Proceedings. Vol. 1647. AIP Publishing LLC, 2015, pp. 44–

    2015

  88. [102]

    Testing coupled dark energy with large scale structure observation

    Weiqiang Yang and Lixin Xu. “Testing coupled dark energy with large scale structure observation”. In:Journal of Cosmology and Astroparticle Physics2014.08 (Aug. 2014), p. 034. doi: 10.1088/1475-7516/2014/08/034 . url: https://dx.doi.org/10.1088/ 1475-7516/2014/08/034

    2014 doi

  89. [103]

    New constraints on inter- acting dark energy from cosmic chronometers

    Rafael C. Nunes, Supriya Pan, and Emmanuel N. Saridakis. “New constraints on inter- acting dark energy from cosmic chronometers”. In:Physical Review D94.2 (July 2016). issn: 2470-0029. doi: 10.1103/physrevd.94.023508 . url: http://dx.doi.org/10. 1103/PhysRevD.94.023508

    2016 doi

  90. [104]

    Testing the interaction between dark energy and dark matter via the latest observations

    Jian-Hua He, Bin Wang, and Elcio Abdalla. “Testing the interaction between dark energy and dark matter via the latest observations”. In:Physical Review D83.6 (Mar. 2011). issn: 1550-2368. doi: 10.1103/physrevd.83.063515 . url: http://dx.doi.org/10. 1103/PhysRevD.83.063515

    2011 doi

  91. [105]

    Dynamics of nonlinear interacting dark energy models

    Andronikos Paliathanasis, Supriya Pan, and Weiqiang Yang. “Dynamics of nonlinear interacting dark energy models”. In:International Journal of Modern Physics D28.12 (Sept. 2019), p. 1950161. issn: 1793-6594. doi: 10 . 1142 / s021827181950161x. url: http://dx.doi.org/10.1142/S02...

    2019 doi

  92. [106]

    url: http://dx.doi.org/10.1063/1.4913335

    doi: 10.1063/1.4913335. url: http://dx.doi.org/10.1063/1.4913335

    doi

  93. [108]

    Observational con- straints and predictions of the interacting dark sector with field-fluid mapping

    Joseph P. Johnson, Archana Sangwan, and S. Shankaranarayanan. “Observational con- straints and predictions of the interacting dark sector with field-fluid mapping”. In:Jour- nal of Cosmology and Astroparticle Physics2022.01 (Jan. 2022), p. 024.issn: 1475-7516. doi: 10.1088/147...

    2022 doi

  94. [109]

    Remedy of some cosmological tensions via effective phantom-like be- havior of interacting vacuum energy

    Suresh Kumar. “Remedy of some cosmological tensions via effective phantom-like be- havior of interacting vacuum energy”. In:Physics of the Dark Universe33 (Sept. 2021), p. 100862. issn: 2212-6864. doi: 10.1016/j.dark.2021.100862. url: http://dx.doi. org/10.1016/j.dark.2021.100862

    2021

  95. [110]

    Quantum field theory of inter- acting dark matter and dark energy: Dark monodromies

    Guido D’Amico, Teresa Hamill, and Nemanja Kaloper. “Quantum field theory of inter- acting dark matter and dark energy: Dark monodromies”. In:Physical Review D94.10 (Nov. 2016). issn: 2470-0029. doi: 10.1103/physrevd.94.103526 . url: http://dx. doi.org/10.1103/PhysRevD.94.103526

    2016 doi

  96. [111]

    Cosmological constraints on parametrized interacting dark en- ergy

    R. von Marttens et al. “Cosmological constraints on parametrized interacting dark en- ergy”. In:Physics of the Dark Universe23 (Jan. 2019), p. 100248.issn: 2212-6864. doi: 10.1016/j.dark.2018.10.007. url: http://dx.doi.org/10.1016/j.dark.2018.10. 007

    2019 doi

  97. [112]

    Testing interacting dark matter and dark energy model with cosmo- logical data

    Gong Cheng et al. “Testing interacting dark matter and dark energy model with cosmo- logical data”. In:Phys. Rev. D102 (4 Aug. 2020), p. 043517.doi: 10.1103/PhysRevD. 102.043517. url: https://link.aps.org/doi/10.1103/PhysRevD.102.043517

    2020 doi

  98. [113]

    Improved cosmological constraints from a joint analysis of the SDSS- II and SNLS supernova samples

    Marc Betoule et al. “Improved cosmological constraints from a joint analysis of the SDSS- II and SNLS supernova samples”. In:Astronomy & Astrophysics568 (2014), A22

    2014

  99. [114]

    Cobaya: Code for Bayesian Analysis of hierarchical physical models

    Jesus Torrado and Antony Lewis. “Cobaya: Code for Bayesian Analysis of hierarchical physical models”. In: Journal of Cosmology and Astroparticle Physics2021.05 (2021), p. 057

    2021

  100. [115]

    Inference from iterative simulation using multiple sequences

    Andrew Gelman and Donald B Rubin. “Inference from iterative simulation using multiple sequences”. In:Statistical science7.4 (1992), pp. 457–472

    1992

  101. [116]

    Tale of stable interacting dark energy, observational signatures, and the H0 tension

    Weiqiang Yang et al. “Tale of stable interacting dark energy, observational signatures, and the H0 tension”. In:Journal of Cosmology and Astroparticle Physics2018.09 (Sept. 2018), pp. 019–019. issn: 1475-7516. doi: 10 . 1088 / 1475 - 7516 / 2018 / 09 / 019. url: http://dx.doi....

    2018 doi

  102. [117]

    A Practical Solution to the Pervasive Problems of p Values

    Eric-Jan Wagenmakers. “A Practical Solution to the Pervasive Problems of p Values”. In: Psychonomic bulletin & review14 (Nov. 2007), pp. 779–804.doi: 10.3758/BF03194105

    2007 doi

  103. [118]

    The Dark Energy Survey: Cosmology Results with 1500 New High- redshift Type Ia Supernovae Using the Full 5 yr Data Set

    TMC Abbott et al. “The Dark Energy Survey: Cosmology Results with 1500 New High- redshift Type Ia Supernovae Using the Full 5 yr Data Set”. In:The Astrophysical Journal Letters 973.1 (2024), p. L14

    2024

  104. [119]

    Bayes factors

    Robert E Kass and Adrian E Raftery. “Bayes factors”. In:Journal of the american sta- tistical association90.430 (1995), pp. 773–795

    1995

  105. [120]

    The Theory of Probability

    Harold Jeffreys. The Theory of Probability. Oxford Classic Texts in the Physical Sciences,

  106. [122]

    GetDist: a Python package for analysing Monte Carlo samples

    Antony Lewis. “GetDist: a Python package for analysing Monte Carlo samples”. In:arXiv preprint arXiv:1910.13970 (2019)

    2019 arXiv

  107. [124]

    Bayes in the sky: Bayesian inference and model selection in cosmology

    Roberto Trotta. “Bayes in the sky: Bayesian inference and model selection in cosmology”. In: Contemporary Physics49.2 (2008), pp. 71–104

    2008

  108. [1939]

    isbn: 978-0-19-850368-2, 978-0-19-853193-7. 16

  109. [2021]

    arXiv: 2111.04629 [astro-ph.CO]

    arXiv

  110. [2025]

    url: https://arxiv.org/abs/2507.13890

    arXiv: 2507.13890 [astro-ph.CO]. url: https://arxiv.org/abs/2507.13890

    arXiv

  111. [4357]

    url: http://dx.doi.org/10.3847/1538- 4357/abe86a

    doi: 10.3847/1538- 4357/abe86a . url: http://dx.doi.org/10.3847/1538- 4357/abe86a

    doi

  112. [8213]

    url: http://dx.doi.org/10.3847/2041- 8213/ab75f0

    doi: 10.3847/2041- 8213/ab75f0 . url: http://dx.doi.org/10.3847/2041- 8213/ab75f0

    doi

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